[1]} show that the absence of mode detection was not an observational bias but a true mode damping.
The shorter the orbital period and the closer the stars are, the weaker the oscillation modes become until complete mode depletion is reached.
These authors observe the damping of modes in systems with an orbital period shorter than approximately 40 days, for which most orbits are circularized and rotation periods are synchronized.
This suppression of mode power confirms the inverse relation between mode amplitude and magnetic activity observed for the Sun and other solar-like stars [2]}, [3]}.
This is further confirmed by [4]}, who show that systems with short circularization timescales have suppressed oscillations.
